Selecting M-giants with infra-red photometry: Distances, metallicities and the Sagittarius stream

TL;DR

This study develops a method using infrared photometry to select M-giants, estimate their metallicities, and determine distances, enabling detailed analysis of the Sagittarius stream's structure and composition.

Contribution

It introduces a new classification for M-giants using WISE and 2MASS data, along with empirical relations for metallicity and distance estimation, improving upon previous model-based methods.

Findings

Efficient separation of M-giants from M-dwarfs using WISE bands.

Strong correlation between (W1-W2) color and metallicity.

Confirmation of the metallicity offset between Sagittarius stream tails.

Abstract

Using a spectroscopically confirmed sample of M-giants, M-dwarfs and quasars from the LAMOST survey, we assess how well WISE $\&$ 2MASS color-cuts can be used to select M-giant stars. The WISE bands are very efficient at separating M-giants from M-dwarfs and we present a simple classification that can produce a clean and relatively complete sample of M-giants. We derive a new photometric relation to estimate the metallicity for M-giants, calibrated using data from the APOGEE survey. We find a strong correlation between the $(W1-W2)$ color and $\rm [M/H]$, where almost all of the scatter is due to photometric uncertainties. We show that previous photometric distance relations, which are mostly based on stellar models, may be biased and devise a new empirical distance relation, investigating trends with metallicity and star formation history. Given these relations, we investigate the properties of M-giants in the Sagittarius stream. The offset in the orbital plane between the leading and trailing tails is reproduced and, by identifying distant M-giants in the direction of the Galactic anti-center, we confirm that the previously detected debris in the outer halo is the apocenter of the trailing tail. We also find tentative evidence supporting an existing overdensity near the leading tail in the Northern Galactic hemisphere, possibly an extension to the trailing tail (so-called Branch C). We have measured the metallicity distribution along the stream, finding a clear metallicity offset between the leading and trailing tails, in agreement with models for the stream formation. We include an online table of M-giants to facilitate further studies.